Rock spatial densities on the rims of the Tycho secondary craters in Mare Nectaris

Basilevsky, A. T.; Michael, G.G.; Козлова, Н. А.

doi:10.1016/j.pss.2018.02.002

Cited by 7 publications

(3 citation statements)

References 9 publications

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“…Previous studies have analyzed the cumulative size frequency of boulders around craters or at landing sites (Bart & Melosh, 2010;Basilevsky et al, 2013Basilevsky et al, , 2015Basilevsky et al, , 2018Cintala & McBride, 1995;Krishna & Kumar, 2016;Li et al, 2017Li et al, , 2018Shoemaker et al, 1969), but few have addressed the distribution of boulders as a function of distance from the crater rim, with the exception of Krishna and Kumar (2016), who analyzed boulder distributions around an oblique impact. Our counts therefore improve upon these studies by determining the maximum distance that craters distribute boulders, how boulder size distributions vary as a function of distance, and how these distributions change as a function of crater size and crater age.…”

Section: Introductionmentioning

confidence: 99%

“…High-resolution Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) images provide the best image data currently available for conducting quantitative boulder counts at these regions. The LROC NACs have obtained the highest resolution images (~0.5-2 m/pixel) of the lunar surface acquired from orbit to date, enabling the use of boulder distributions for a variety of purposes (e.g., Bandfield et al, 2011;Bart & Melosh, 2010;Basilevsky et al, 2013Basilevsky et al, , 2015Basilevsky et al, , 2018De Rosa et al, 2012;Jawin et al, 2014;Krishna & Kumar, 2016;Lawrence et al, 2013;Li et al, 2017;Watkins et al, 2017).…”

Section: Introductionmentioning

confidence: 99%

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Boulder Distributions Around Young, Small Lunar Impact Craters and Implications for Regolith Production Rates and Landing Site Safety

et al. 2019

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We use Lunar Reconnaissance Orbiter Camera Narrow Angle Camera images to characterize boulder populations around six small (<1 km), young (<200 Ma) impact craters near spacecraft landing sites. The Narrow Angle Camera boulder counts are used to analyze how boulder distributions vary around craters of different sizes and ages. These comparisons inform how various properties affect the distance to which boulders are ejected and the size and density of boulders produced by an impact event. The counts show that boulder population densities decrease with crater age, with few boulders remaining at craters older than a few hundred million years, consistent with results of other studies of boulder degradation rates on the Moon. Variations in boulder distributions around younger craters may provide information regarding impact conditions; South Ray crater has a larger population of small boulders than the larger North Ray crater, which could be explained by variations in impact velocity. Large craters generally excavate more boulders than smaller craters, and the size of the largest boulder ejected is related to crater size by a power‐law function. Larger boulders occur closer to the crater rim (within 2–4 crater radii), whereas smaller boulders occur at all distances. The density of boulders is greater near the crater rim and decreases with increasing radial distance; this data can aid in establishing safe landing zones for future missions. Analyzing boulder distributions across craters of varying ages allows us to test models of boulder breakdown rates, with implications for understanding the Moon's regolith production rate.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Boulder Distributions Around Young, Small Lunar Impact Craters and Implications for Regolith Production Rates and Landing Site Safety

et al. 2019

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“…Several fundamental questions on the physical properties of impact craters have been addressed based on these advanced data sets. For example, the formation and degradation mechanisms of radar bright halo and dark halo craters (e.g., Gupta & Ghent 2008;Ghent et al 2010Ghent et al , 2016, the distribution characteristics and age of radar anomalous craters (e.g., Fa & Cai 2013;Eke et al 2014;Fa & Eke 2018), the survival time of rocks and boulders on the lunar surface (e.g., Basilevsky et al 2013Basilevsky et al , 2015Basilevsky et al , 2018, and the dating of individual impact craters (e.g., Bell et al 2012;Ghent et al 2014;Li et al 2018). Furthermore, the temporal evolution of radar circular polarization ratio (CPR) was investigated based on a mare crater database (800 m-5 km; N = 13 657; King et al 2017;Fassett et al 2018a;Nypaver et al 2019Nypaver et al , 2021.…”

Section: Introductionmentioning

confidence: 99%

Evolution of Subkilometer-scale Impact Craters on the Lunar Maria as Constrained from Mini-RF Data and Topographic Degradation Model

Sun 孙,

Fa 法,

Zhu 祝

et al. 2023

Res. Astron. Astrophys.

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Physical properties (e.g., ejecta size and distribution) of impact craters are crucial and essential to understand ejecta excavation and deposition process, estimate rock breakdown rate, and reveal their the evolution characteristics. However, whether these physical properties are scale-dependent and how they evolve in different radial regions need further studies. In this study, we first investigated the physical properties and evolution of sub-kilometer (D ≤ 800 m) craters on lunar maria based on the radar circular polarization ratio (CPR). In addition, we estimated the periods over which rocks and blocky ejecta are exposed and buried in the shallow subsurface layer (termed as exposure time) in different radial regions and assessed the retention time and degradation states for potential radar anomalous craters. We found that in the central region of craters, the largest median CPR occurs after an 80 Myr delay following crater formation. In the rim region, there is no obvious CPR peak in the first 100 Ma, whereas in the upper wall region, evident CPR peak occurs beyond 100 Ma and could last over one billion years. In addition, the probable exposure time of rocks and blocky ejecta are estimated to be ∼2.0 Gyr (central region), ∼2.7 Gyr (upper wall region), ∼2.1 Gyr (rim region), and ∼0.6 Gyr (continuous ejecta blanket region). We also propose that the retention time of radar anomalous craters depends on the crater size, whereas their degraded states are independent on crater size.

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A reanalysis of the relationship between the size of boulders and craters in lunar surface

Jia

Yue

et al. 2019

Icarus

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Rock spatial densities on the rims of the Tycho secondary craters in Mare Nectaris

Cited by 7 publications

References 9 publications

Boulder Distributions Around Young, Small Lunar Impact Craters and Implications for Regolith Production Rates and Landing Site Safety

Boulder Distributions Around Young, Small Lunar Impact Craters and Implications for Regolith Production Rates and Landing Site Safety

Evolution of Subkilometer-scale Impact Craters on the Lunar Maria as Constrained from Mini-RF Data and Topographic Degradation Model

A reanalysis of the relationship between the size of boulders and craters in lunar surface

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